Titlebook: Chromospheric Fine Structure; R. Grant Athay Book 1974 International Astronomical Union 1974 Chromosphere.Corona.LOPES.Sunspot.solar.sun

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書目名稱Chromospheric Fine Structure影響因子(影響力)




書目名稱Chromospheric Fine Structure影響因子(影響力)學(xué)科排名




書目名稱Chromospheric Fine Structure網(wǎng)絡(luò)公開度




書目名稱Chromospheric Fine Structure網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Chromospheric Fine Structure被引頻次




書目名稱Chromospheric Fine Structure被引頻次學(xué)科排名




書目名稱Chromospheric Fine Structure年度引用




書目名稱Chromospheric Fine Structure年度引用學(xué)科排名




書目名稱Chromospheric Fine Structure讀者反饋




書目名稱Chromospheric Fine Structure讀者反饋學(xué)科排名

木質(zhì)

Book 1974rk phenom- ena and to ascertain the physical properties of the network features. Clearly, the supergranule cells and associated network structures constitute a fundamental and singularly important feature of solar structure in the boundary layers. Just as it is now clear that much of the chromo sphe

intrigue

1743-9213 ctures constitute a fundamental and singularly important feature of solar structure in the boundary layers. Just as it is now clear that much of the chromo sphe978-90-277-0288-3978-94-010-2103-6Series ISSN 1743-9213 Series E-ISSN 2352-2186

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Radiation Pressure in Stellar Atmospheres with Application to Solar Spiculesthe network areas the pressure gradient due to radiation is comparable to (and oppositely directed to) that due to gravitation and that in local areas of unusual brightness the net pressure gradient is outwards. An estimate of the expected outwards velocity of spicule material driven by radiation pr

慎重

Neue Denkweisen statt wechselnde Konzeptemetric either for the whole line or for fine structure. The quality of the data is such as to improve our understanding of line blends. The spectral structure can be compared with the well-known structure in the H and K lines of Ca it and in the resonance lines of Mg it in order to deduce a model for the lower chromosphere.

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Neue Denkweisen statt wechselnde Konzepteg H. ± 2 ?) and even into the continuum. They called this fine structure ‘solar filigree’, the name referring mainly to the collective appearance of the fine structure elements. The elements themselves appear as dot-like structures and frequently also as small wiggly structures called ‘crinkles’.

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Michele Averchi,Emanuele Colombotude against the projected baseline at the time of the event suggests emission from a region of angular size of about 10″. The corresponding brightness temperature is 50000 K. It is possible that these events may be related to the appearance and disappearance of groups of spicules or mottles.

chance

stress-test

Spatial and Spectral Structure of Chromospheric Linesmetric either for the whole line or for fine structure. The quality of the data is such as to improve our understanding of line blends. The spectral structure can be compared with the well-known structure in the H and K lines of Ca it and in the resonance lines of Mg it in order to deduce a model for the lower chromosphere.

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